NCAR/TN-213+STR the Second Joint Solar Dynamics Project Data

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NCAR/TN-213+STR NCAR TECHNICAL NOTE _ I I I -I 1~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~ July 1983

The Second Joint Solar Dynamics Project Data Summary

Solar Magnetic Field, Chromospheric and Coronal Observations Near the Time of the 11 June 1983 Solar Eclipse

D.G. Sime, R.R. Fisher, C.J. Garcia, J.R. Najita, K.A. Rock, P.H. Seagraves, and E.A. Yasukawa, NCAR

M.K. McCabe and D.L. Mickey, University of Hawaii

HIGH ALTITUDE OBSERVATORY I ~~~~~~-- NATIONAL CENTER FOR ATMOSPHERIC RESEARCH BOULDER, COLORADO

iii

CONTENTS

page

PREFACE v.

I. INTRODUCTION . 1

II. MLSO DATA PRODUCTS 4

III. MSO DATA PRODUCTS 8

IV. DATA COVERAGE 11

V. SOLAR ACTIVITY DURING THE SOLDYN II PERIOD 13

VI. DAILY SOLAR DATA 17

VII. SYNOPTIC SOLAR DATA 51

ACKNOWLEDGMENTS 57

REFERENCES 59

PREFACE

The success of the first Joint Solar Dynamics Project (SOLDYN I) observing period (see NCAR Technical Note TN-202+STR and Fisher et al., 1983) demonstrated the power of the integrated operation and co-ordination of instruments available in the Hawaiian islands in producing a wide-ranging observational record of conditions on the sun. Examination and analysis of the data collected made it clear that this instrumentation would also allow the collection of a valuable record of the sun near the time of the 11 June 1983 solar eclipse. Such a record would be valuable to the High Altitude Observatory (HAO) and University of Hawaii (U of H) eclipse expedition scientific analysis efforts, and would also provide a valuable context for the community at large in which to interpret its own eclipse observations. Further, the observations would give an opportunity to verify whether the observed relationships established during SOLDYN I were maintained on the sun a year later in the solar cycle.

At a planning meeting which took place on 18 April 1983, during the 3rd

Hawaiian Neighborhood Meeting in Honolulu, the decision was made to carry out these co-ordinated observations under the name SOLDYN 11. This Technical

Note presents the observations made during this effort in the interval 3-17 June

1983. As far as possible, daily observations made with the Mark-Ill k- coronameter of the Mauna Loa Solar Observatory (MLSO) as well as photographic records of the sun in Ca II and Ha, and from the flare patrol at Mees

Solar Observatory (MSO) on Haleakala, Maui, are included. We also present daily observations of the longitudinal component of the photospheric magnetic field made at MSO. Finally, the coronal and magnetic field observations are assem- bled into synoptic maps for the period near the eclipse.

D. G. Sime, July 1983

High Altitude Observatory I. INTRODUCTION

The general goal of the HAO/University of Hawaii Joint Solar Dynamics Pro- ject is to establish the relationships that exist between the solar magnetic field as detected in the photosphere and the structure and evolution of the corona.

The SOLDYN program of 19B2 (see Fisher et al., 19B2a) demonstrated our ability to use existing instruments to gather data of value in the pursuit of that goal.

During that program, which ran from 14 June to 13 August 1983, daily co- ordinated observations were made of the sun and corona using the Mark-111 k- coronameter and the prominence monitor at HAO's Mauna Loa Solar Observa- tory (MLSO) and the Stokes polarimeter, Ha flare patrol and Ca II cameras, and the Ha coronagraph at U of H's Mees Solar Observatory (MSO). This wide ranging record of the sun enabled us to begin to address specific questions in par- tial satisfaction of our goal (Fisher et al., 1983) and encouraged us to believe that additional observations in the summer of 1983 would be of value. Specifi- cally, these new data would allow us to achieve three ends:

(1) Document the state of the sun, from the photosphere up through the chro-

mosphere and out into the corona for the two week period around the total

solar eclipse of 11 June 1983,

(2) Specify the relationship between the photospheric magnetic fields and the

temperature and density structure of the corona, and

(3) Verify the relationship between inferred coronal mass and the observed Ca

II K-line plage area which was established during the SOLDYN project.

In this NCAR Technical Note, we present the reduced observations made

during the SOLDYN II period and necessary to achieve these goals. They are

presented both in the form of daily photographic and photo-electric measure-

ments, and in synoptic format for the period. 2

To satisfy the scientific requirements of the program, the following comrple- ment of observations was defined for each day:

Mees Solar Observatory (MSO):

(1) One Stokes polarimeter scan of the center third of the disk at XG3Jo3

(2) One Ca 11 K-line, 0.3A FWHM filtergram of the full disk

(3) One Ha, 0.5A FWHM, on-band filtergram of the full disk

(4) One Ha, 0.5A FWHM, off-band filtergram of the full disk, AkX-A1

(5) One Ha, t 7.6A FWHM, full-limb image

Mauna Loa Solar Observatory (MLSO):

(1) One contour plot of the inner coronal pB distribution as a function of posi-

tion angle and height from 1.3 to 2.1 Jo

(2) Two plots of inferred pB as a function of latitude and longitude, called

SHELL, for heights above the limb of 1.3 fP and 1.7 /Ki

(3) One daily DIMAGE difference image plot, a subtraction of the previous day's

synoptic pB image from the present day's data.

(4) One Ha, 0.5X FWHM, disk image (back-up only).

(5) One Ha, B.1A FWHM, full-limb image (back-up only).

In addition to the daily central disk scans with the Stokes polarimeter, on the 10th and 12th of June, extra scans, encompassing the West (on the 10th) and the East (on the 12th) limbs, were made.:

In spite of the varied and changeable observing conditions, the skill and perseverance of the two observatory site crews paid off in an almost complete set of observations. The full basic daily set of data was achieved on 1.4 out of 15 days; a tribute to the effectiveness of both individual and team efforts. Both 3

sites were active on 100% of SOLDYN II observing days as shown in Table 2. The sky was generally clearer for these observations than it was last summer, and the weather was generally fair, providing favorable observing conditions on the whole, particularly in the mornings.

The sun was not particularly active during these observations, and the active regions which we observed were quite well spread out over the entire sun, in contrast to last year's conditions. No coronal transients were observed either during Mark-111 operations or by deduction from the daily DlVIAGE. On the final day of operations for SOLDYN II, a large EPL event occurred on the

Southeast limb, but no observed coronal transient was associated with it. The limb at eclipse time seemed rather quiet. The activity noted by the observers is summarized in Table 3. 4

II. MLSO DATA PRODUCTS

The observations carried out at MLSO provided 2 data sets; photo-electric measurements of the polarized coronal radiance, and photographic records of the limb and disk of the sun.

Mark-Ill

The Mark-ll k-coronameter is a 23 cm diameter objective iadging k- coronameter, which produces digital images at the rate of three images every

184 s. This system has been described by Fisher et al. (1961), and is the major piece of instrumentation at MLSO. Digital images are recorded onto 1,600 bpi nine-track magnetic tape. During the SOLDYN II period, three types of reduced data were produced. These were:

(1) A calibrated contour plot of the coronal pB distribution (1MAP)

(2) Two inferred coronal pB distributions plotted onto spherical projections,

one each for heights of 1.3 Jo and 1.7 fJo (SHELL)

(3) Contour plots of the daily one-day difference pB distribution (DIMAGE).

For more discussion of these data products, the reader is directed to the discussion by Rock and Seagraves (1982); some more detail is given below.

P-MON

The prominence monitor at MLSO is an internally occulted telescope which is used to observe the sun's limb, and which provided the photographic data from MLSO. A solar image, 11.5-mm in diameter, is recorded on 35-mm SO-2415 film giving a plate scale of 166.9 arc seconds/mm. The Ha disk is observed by using a Ak FWHM X6563 filter. The observing format used is a three frame graded sequence of an under-, nominal- and over-exposed image of the limb through an B.1A FWHM interference filter usually followed by a single disk image. Several pauses are programmed into the routine to allow the observer to view the sun with the television camera for activity awareness. One loop of the film sequence requires 4 min to complete. This monitoring program was run continuously from about 1 h after dawn until shutdown at approximately local noon. The MLSO crew was able to operate the prominence monitor 14 days out of the 15 days of the solar dynamics observing program.

1MAP

The 1MAP program became part of the MLSO observing procedure on 31

January 1982. It replaces all previous coronal mapping programs for the daily data archive. The map is proportioned to agree with the instrument's actual field of view, which extends roughly between 1.2 and 2.1 fiP. To give an irnmmedi- ate idea of the coronal pB amplitude, there is a single polar plot of pB in the center of the graph, which is taken at the height of 1.35 Ro. For this plot, the center is the zero pB level, and the inner circle is at the 20 pB level. Units of pB are given in units of 10- 8E (percent polarization), where Bo is the mean brightness of disk center at the effective wavelength of 8200A.

SHELL

SHELL plots are drawn from data that represent a single height in the corona. Each day, a scan is taken from which the data at three heights are extracted and simultaneously recorded onto the systems disk. This represents a small portion of the daily data taken; however, it permits convenient long- term storage of data in a limited area of the systems disk. These data have been collected since 8 August 1980. The data are reproduced on a contour map corrected for its position in the sky for a one-half rotation period.

These plots may be used for prediction to determine where and when coronal activity, which is likely to be present above active regions, might appear at either limb. It may also be used to comnare with solar photographs for any requested time if placed over an appropriately sized solar image. The East limb 6

plot for DOY N will show the distribution of coronal material as seen from the earth on DOY N.

DIMAGE

MLSO uses a differencing system to detect changes in the corona. Two images are stored on the system disk of the control computer and the first image is subtracted from the second. The results are presented as a contour plot. All features present in both images disappear, leaving only the changes that have occurred. Depletions are drawn in solid contour lines. Enhance- ments (areas where the corona has grown brighter) are drawn in dashed contour lines. This plot will also show fluctuations in sky polarization and system noise. Using DIMAGE, the observer is able to interpret accurately the activity level in near real time. Plots that show significant changes are archived in Hilo.

Used on line, this procedure can take as little as 10 min. At some point during the observing period, the observer selects the best image for the day. A difference plot is made with the corresponding image from the previous day. These daily difference plots are of interest because they are one way of inferring transient and evolutionary coronal changes over a variety of time scales ranging from 6 min to one day.

The DIMAGE plot is uncorrected for instrumental effects, most. notdably the effect of a triangular sample slit, but it is possible to interpret this real-time data plot with the help of Table 1. In the first three columns, height above the limb is given in units of the fractional height of the field of view in the DIMAGE plot, height in arc seconds, and in units of Po above the true limb of the sun. As many as three contours may be plotted on the DIMAGE map. Depleted regions are indicated by a solid contour line. The absolute value of the inferred difference in pB detected is actually a function of height due to the triangular sample slit and the vignetting of the lower corona by the occulting disk. This varia- 7

-- columns four through six in Table 1. Thus, an indication of a depleted region enclosed by two solid contours at midpoint between the limb and the edge of the field of view implies a ApB between 2.4 x 10-8 Bo and 3.7 x 10-8 1 has occurred between the two images used to estimate the DIMAGE plot. More infor- mation concerning the DIMAGE plot is given by Rock and Seagraves (1962).

TABLE 1

ApB vs Height

Height Contour Levels (x 10 - 8 £) r(fractional h(arc sec) fi 1st 2nd 3rd height in DIMAGE)

0.0 350 1.36 1.9 3.8 5.7

0.5 710 1.73 1.2 2.4 3.7

1.0 1160 2.20 0.7 1.6 2.4 8

Ill. MSO DATA PRODUCTS

The synoptic program conducted at MSO on Haleakala for SOLDYN II was

directed toward obtaining two distinct but related sets of observations.

The first, photo-electric series, using the Haleakala Stokes polarimeter

(see Mickey and McCabe, 1963), was designed to lead to vector magnetic field and line of sight velocity measurements in the photosphere. The second set of observations consists of complementary photographic observations of the chromosphere and photosphere as well as of limb prominences for correlation and comparison with the white light coronal structure.

Stokes polarimeter

The Haleakala Stokes polarimeter consists of a 15-cm aperture, f:16 telescope with a pinhole field stop at the prime focus, a rotating quarter-wave plate retarder, and a compact high-resolution echelle spectrometer. A 126-element detector array in each of the two beams at the spectrometer focus provides simultaneous recording across a 3A spectral range. The polarimeter produces line profiles in each of the Stokes parameters I, Q. U. V, which are displayed in real time for the observer and stored on magnetic media for off-line processing.

The magnetically sensitive line selected for this study was Fe I Xf6302.5, a simple triplet with an equivalent width of 80rmA and a lower-level excitation potential of 3.67eV. The line is free from blends, and there are telluric 02 lines at X6302.0 and X6302.76 which can be used as references for velocity determi- nations. The pinhole and spectrometer entrance slit were chosen to provide a field of 30 x 3.7 arcsec and a geometrical instrumental width of 60rnA. Pixel separation in the detectors is approximately 25rnX at this wavelength.

For each day, data were obtained for approximately 1400 spatial points in a rectangular raster centered on the solar disk. The raster covered the full solar diameter in the (geocentric) north-south direction, and 610 arcsec east-west, 9

with a point spacing of 29 arcsec. The full raster took approximately 50 minutes to complete when operation could be continuous. Integration time at each point was 0.8 s; the remaining time was consumed by telescope and retarder moves, and by on-line data manipulation. On the days imrrimecdiately before and after the eclipse, an additional scan of similar extent was made cov- ering the West and East limbs respectively to provide the most timely observations of the field below the corona seen during the eclipse.

An empirical magnetic field determination was made at each dala point as follows. The center and FWHM of the iron line were found; the blue and red com- ponents of the V profile were integrated from line center to 1.5 FViHM and differenced. The result was divided by the integral of the intensity profile over

+/- 0.5 FWHM, and multiplied by an empirical factor which has been found to give good agreement with Unnoh-model line fitting procedures for fields below

500G (Elmore, 1982).

To date, the data have been reduced, as presented in this Technical Note, to provide the longitudinal component of the photospheric magnetic field. Work is continuing to derive vector magnetic fields and photospheric line of sight velocity distributions as well.

Flare Patrol

The flare patrol telescope, using an Ha birefringent filter with a 0.5A band pass, monitored the full disk recording a 14-mm solar image on 35-mm film. It ran continuously during the polarimeter scan at a rate of one exposure every

10 min, but had the capability, during periods of flare activity, to have the rate increased to as much as 10/min. Following the scan, exposures were made with the filter tuned off-band to display better any sunspot groups; then a set of graded exposures was taken for calibration purposes and to show prominences on the longer exposures. The filtergrams in this year's data required generally 10

shorter exposures than last year's since the effect of the volcanic cloud was less pronounced in our sky this year (see Garcia and Yasukawa, 1983).

Ca II K-line Telescope

The Ca II K-line telescope is optimized for use at X3934 and employs a birefringent filter with a band pass of 0.3A to produce solar images 45D-mm in diameter in the K-line. Photographs on 70-mm film were obtained under manual control with at least one set of three exposures (1-2 sec) recorded each observing day. The telescope is mounted on a 45° face of the spar, so the images have been reoriented in the data set to have the same orientation as the other filtergrams.

Red Coronagraph

The red coronagraph is a telescope with a 10-cm aperture which is used to record the solar corona in Hc, around the entire solar limb. The Hoc interference filter has a band pass of 7.5Y and the image is recorded on 70-mm film with a diameter of 38-mmrn; a set of exposures (1/2, 1, and 2 sec) was taken at least once each day, and more frequently during any limb activity. Note that on days when Ha coronagraph observations were not available from. MSO, we have presented the prominence monitor images from MLSO. 11

IV. DATA COVERAGE

A coverage list, Table 2, summarizes the combined operations of the joint project. The times during which each instrument operated are logged as a function of date and day of year (DOY). All times are in U.T. The V-designation

(NCAR data tape volume number) is given for all Mark-Il1 observations.

TABLE 2 SOLDYN 1 DATA COVERAGE

DATE(DOY) POLARIMETER PHOTOS MLSO SCAN Flare Patrol R. Cor Ca K-line P-MON Mark-ill Mag Tape ___

June 3 (154) 1758 1759-1836 1755-1820 18:09:43 V67315 18:12:45

4 (155) 1819 1730-1937 1936 1739-1748 1815-1909 18;42:18 V67315 +ob,gs 18:45:20

5 (156) 1818 1728-1930 1944 1738-1741 1815-1835 18:20:56 V67318 +ob,gs 18;24:00

6 (157) 1822 1816-1947 1944 1941 1828-2203 18;50:37 V67318 +ob,gs 18:53:41

7 (158) 1746 1733-1915 2051 1916 1911-2130 21:17:32 V67318 +ob,gs 21:20:40

8 (159) 1920 1727-2034 2125 2120 1815-2156 18:38:37 V67318 2105 ob,gs 18:41:40

9 (160) 2334 1845-1925 2048 1846-2053 1831-2144 18:41:09 V6731 8 1950-2125 18.44;14

10 (161) 1937 1716-1818 1748 1812-1817 1815-0045 18:29:30 V67318 1820 ob,gs 2043-West Limb 1827-0426 1834 18:32:34 0011 0222 0306 0430

1 (162) 1753 1704-1958 1708 1717 +ob,gs

ob=90 degrees off band gs = long graded set with sector shutter set at 160.0, 110.0, 85.0 12

DATE(DOY) POLARIMETER 6303 PHOTOS MLSO SPECTROHELIOGRAM Flare Patrol R. Cor Ca K-line P-MON MARTK- II ]iagg Tape

II II -

12 (163) 1830 1717-2047 1756 1747-1750 1829-1853 18:35:51 V6731 1944-East Limb +ob,gs 18:38:55

13 (164) 1750 1723-2020 2032 2131-2035 1814-2159 18:22:35 V67316 +ob,gs 18:56:17

14 (165) 1800 1754-1930 2043 1940 1758-2159 18:31:32 VC7323 +ob,gs 18;34'57

15 (166) 1743 1738-1854 1911 1909 1802-2205 18:32:06 V67323 +ob,gs 18:35:12

16 (167) 1854 1847-2002 2009 2006 1755-2039 18:52:10 V\67323 +ob,gs 18:55:16

17 (168) 1808 1729-1911 1917 1922-1919 1812-2120 18:56;53 V67323 +ob,gs 1952 18:59:59

ob=90 degrees off band gs = long graded set with sector shutter set at 160.0, 110.0, 85.0 13

V. SOLAR ACTIVITY DURING THE SOLDYN II PERIOD

As an aid to the reader, a short summary of solar activity detected by us

during the observational phase of the project is given below in Table 3. This list is not intended to be a comprehensive specification of the level of activity, but it merely reflects that fraction of the total activity captured in the joint project data set. There is a short comment concerning the specific limb events observed; the approximate maximum height above the limb and heliocentric position angle are given as a function of date, DOY, and U.T. A general commient concerning disk activity is also included for each DOY. The limb activity summary is taken from the MLSO prominence monitor real-time video data and the

P-MON automatic log book. TABLE 3 SOLAR DYNAMICS II ACTIVITY LIST

TIME - UT PA RV DATE DOY ACTIVITY 115-125 1.05 Prominence 1742-1906 06-03-83 154 Active 120 1.0.3 Active Region 135 1.0 Quiet Prominence 225-235 1.05 Quiet Prominence 218-232 1.1 Active Region 1755-2005 06-04-83 155 118 Limb Surge Small 35 Quiet Prominence 105 108 258 267

Disc 1818 UT 06-05-83 156 Possible Flare Near Center of * Note: Broken clouds prevented look at Prominences 265 1.0 Active Prominence (Tiny) 1823-2228 06-06-83 157 235 0.4 Active Region 40 1.05 Quiet Prominence 130 1.0 Quiet Prominence 315 1.0 Quiet Prominence 1744-2237 223 06-07-83 158 Quiet Prominence 290 322

1801-2206 52 06-08-83 159 Quiet Prominence 136 226 272 297

* Small Prominences Only on Limb Active Region on Disc 2 Days Away from SW Limb 1.15 Prominence (Almost Eruptive) 1755-2152 220-225 06-09-83 160 Active 110 0.3 Active Region 0.9 Active Region 250 SOLAR DYNAMICS II ACTIVITY LIST (continued)

DATE DOY ACTIVITY TIME - UT PA RV 06-09-83 160 Quiet Prominence 140 1.0 Quiet Prominence 240 1.0 06-10-83 161 Active Prominence 1758-0047 (ECLIPSE 221-226 1.05 DAY) Active Prominence (Small Surges) 241 Quiet Prominence 119 229 296 06-11-83 162 Prominences Visible Through Cirrus 1758-1955 122 255 06-12-83 163 Possible Limb Flare at 1831 1829-2028 128 Small Bright Features 148 285 06-13-83 164 Small Bright Features Active Prominence 1814-2315 125 Small Feature Active Prominence 115 Quiescent Prominence 55 n Large Filament Near Center of Northern Half of Disc

06-14-83 165 Active Prominence 1756-2209 68-80 1.05 Active Prominence 112 1.0 Surge 65 1.1 Quiet Prominence 120 1.0 Quiet Prominence 278 1.0 06-15-83 166 Active Prominence 1800-2315 60-80 Bright 1.0 Prominence 110 1.0 Prominence Developing 235 1.0 Nice Filament 350 0.8 06-16-83 167 Active Prominence 1753-2134 250-255 1.0 Quiet Prominence 68 1.0 Quiet Prominence 77 1.0 Quiet Prominence 102 1.0 Quiet Prominence 132 1.0 Quiet Prominence (Suspended Cloud) 230-240 1.05 Quiet Prominence 305 1.0 SOLAR DYNAMICS II ACTIVITY LIST (continued)

DATE DOY ACTIVITY TIME - UT PA RV

06-17-83 168 Active Prominence 1758-2144 238 1.05 Large Active Prominence (grew during 113-137 morning to 1.2 RV at 2035 UT when it became diffuse and disappeared) Quiet Prominence 41 83 100 249 304 17

VI. DAILY SOLAR DATA

The data recorded during the SOLDYN II observations are presented on the

following pages in a format which uses two facing pages per DOY, as indicated in

Fig. 1. The date and DOY are indicated on the right-hand page. Observations of

the photosphere and chromosphere are on the even-numbered (left-hand)

pages, while the corresponding coronal data are presented on the odd-

numbered (right-hand) pages. The even-numbered pages contain the solar

data as described in Section III, with the top left image showing the HaIx sunll, and

the image on the top right showing the limb patrol in Ha. The frame at the

lower left is the sun in Ca II (X3934) and at lower right an off-band Htx sunspot

image is presented. In the center at the middle of the page is the daily mag-

netic field observation shown as a strip of data superimposed on the part of the

disk of the sun scanned that day. Dark areas represent positive field. All images

are oriented with geocentric north at the top.

The odd-numbered pages contain the coronal data described in Section II, with the 1MAP shown at the top left and the daily DIMAGE shown at top right.

The lower left frame contains the SHELLs produced for observations at 1.3 fP, while the lower right frame contains the SHELLs for 1.7 fi. Fig. I. Page Layouts Even-numbered Pages

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VII. SYNOPTIC SOLAR DATA

For understanding the large scale structure of the corona, synoptic maps may be more helpful than the individual daily observations. Here we present such maps, both of the photospheric magnetic field, and of the coronal distribution of polarized white light radiance.

The magnetic field maps have been created by mapping successive swaths of observations derived from the daily scans onto the rectangular projection displayed. Where more than one observation occurs for a given location, the several observations have been averaged. The maps presented contain only data from the central scan and do not involve any data from the near-limb scans close to the time of the eclipse. To this end, the co-ordinates of each point have been converted to Carrington latitude and longitude, and data (in some cases from several days' observations) have been weighted by cos4 (L-Lo), where

L-L o is the distance from the central meridian at the time of the observation, before being added into the synoptic map file. The map as shown here represents weighted averages for each two-degree interval in latitude and longitude.

The synoptic representation of the white light corona has been fcrmed by mapping the daily limb scans onto a rectangular map, with the day lllnumbers of limb passage marked. This procedure is the same as that described in Fisher et al., 1982b, with the exception that the data is now presented with cross hatch- ing to emphasize the contour levels. Maps formed from both East and West limb passages are presented, and are shown for both the inner (1.3 7 ) and middle

(1.7 &) corona with the day number of limb passage indicated.

SYNOPTIC MAGNETIC FIELD MAP CARRINGTON ROTAT ION 1736 1735 WW -----,

UJ (A

9Q--0°------180° 270° 360° 90O LONGITUDE 54

HIGH ALTITUDE OBSERVATORY MAUNA LOA MK mI K-CORONAMETER HEIGHT= 1.3 Re EA. 3T LIMB NORTH .~~~~ a ~ I +90 -

-90-i SOUTH

WEST LIMB NORTH +90 -

I- In 0- 0I

-90- SOUTH MAY-JUNE 1983 ECLIPSE: DOY 162 55

HIGH ALTITUDE OBSERVATORY MAUNA LOA MK m K-CORONAMETER HEIGHT = 1.7Re EAST LIMB NORTH +90 -

..... _ . , P '"i ~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~ ...... ·. ,.,.~~~~~~~~~~~~~~~~~~~~~~~~~~~~...... __~~~~~~~..... ^T..._....----.----_ w

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ACKNOWLEDGMENTS

This work was supported in part by a grant to the Institute for Astronomy, by the National Aeronautics and Space Administration, grant number NGL 12-

001-011. MLSO is operated by NCAR under sponsorship of the National Science

Foundation. One of us, JRN, was supported by the HAO Summner Undergraduate

Programrr We gratefully acknowledge the support of J. T. Jefferies, director of the Institute for Astronomy, University of Hawaii, and R. M. MacQueen, director of the High Altitude Observatory. The authors wish to thank Cheryl Baker who provided the joint project with secretarial support services from HAO's Kilo support base, C. Semmer and the NCAR photographics group who provided photographic processing support, and Gail Moran who assisted with the final manuscript preparation. Editorial services, and invaluable advice concerning the production of this technical note, were provided by C. Rasmussen of NCAR's

Publications Office.

REFERENCES

Elmore, D., private communication, 1982.

Fisher, R., R. Lee, R. MacQueen, and A. Poland, New Mauna Loa coronagraph sys-

tems. Appl. Opt. 20, 1094-1101, 1981.

Fisher, R. R., C. J. Garcia, K. A. Rock, P. H. Seagraves, E. A. Yasukawa, M. K.

McCabe, D. L. Mickey, J. R. Najita, J. R. Lieberman, and M. G. Hardy, Joint

solar dynamics project data summary 14 June - 13 August 1902, Volumnze I:

chromospheric and coronal observations. Technical Note NCAR/TN-202

+STR, NCAR, Boulder, Colorado, 149 pp 1982a.

Fisher, R., C. Garcia, K. Rock, P. Seagraves, and E. Yasukawa, Ihe whit-e light

solar corona, an atlas of k-coronameter synoptic charts August 1980 Sep-

tember 1981. Technical Note NCAR/TN-188 +STR, NCAR, Boulder, Colorado, 119 pp 1982b.

Fisher, R. R., M. K. McCabe, D. L. Mickey, P. H., Seagraves and D. G. Sime, The sun

as a star, submitted to Astrophys. Jour., 1983.

Garcia, C. J., E. A. Yasukawa, Mauna Loa sky conditions, bench mark and

present, Proc. Astron. Soc. Pacific, in press 1983.

Mickey, D. L., and M. K. McCabe, in preparation, 1983.

Rock, K., and P. Seagraves, A User's Guide to the Mauna Loa Solar Observatory's

Coronal Data System. Technical Note NCAR/TN-200 +STR, NCAR, Boulder,

Colorado, 23 pp. 1982.